GR and EQG results for magnifications, and the time delays of first and second order relativistic images are presented in Tables REF  and REF , respectively. First (Second) order relativistic images are produced after the light winds, once (twice) around the black hole before reaching the observer [1]}. Here noticeable differences with the corresponding results in ECG [2]} are now apparent, with values of
\((\tau _{2p}-\tau _{1p})\)  differing by as much as \(30\%\)  and of \(\mu _{2p}\)  by close to a factor of 2.
The angular position of relativistic images \(\theta _{1p}\) , \(|\theta _{1s}|\) , \(\theta _{2p}\) , and \(|\theta _{2s}|\)  are almost independent of angular source positions. In EQG their values are about 13 and 4 nanoarcseconds less than their corresponding values in GR for first and second order relativistic images respectively, an effect too tiny to be observed with today's telescopes, especially since these relativistic images are highly demagnified.
However once technology develops the renders them observable, (differential) time delays of relativistic images could be used to test both EQG and ECG, because of their increasing deviation from GR for large \(\beta \) , as can be seen from Tables REF  and REF .
